Are inflationary predictions sensitive to very high energy physics?

Burgess, C. P.; Cline, James M.; Lemieux, François; Holman, R.

doi:10.1088/1126-6708/2003/02/048

Cited by 161 publications

(220 citation statements)

References 32 publications

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“…Any other particular choice would be a strong assumption to be justified. The only simplification that one may consider is to assume that x k ≃ x Let us notice that superimposed oscillations could also originate from other physical mechanisms [121,122,123,124,125] and y k ∼ y, that is to say that these two coefficients are not strongly scale dependent in the range of scales under consideration. In the following, the parameters x and y are considered as free parameters that are not fixed by any existing well-established theories except that, of course, they should satisfy |c k | 2 − |d k | 2 = 1.…”

Section: Basic Equationsmentioning

confidence: 99%

Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data

Martin

Ringeval

2006

J. Cosmol. Astropart. Phys.

242

374

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Abstract.The implications of the WMAP (Wilkinson Microwave Anisotropy Probe) third year data for inflation are investigated using both the slow-roll approximation and an exact numerical integration of the inflationary power spectra including a phenomenological modelling of the reheating era. At slow-roll leading order, the constraints ǫ 1 < 0.022 and −0.07 < ǫ 2 < 0.07 are obtained at 95% CL (Confidence Level) implying a tensor-to-scalar ratio r 10 < 0.21 and a Hubble parameter during inflation H/m Pl < 1.3 × 10 −5 . At next-to-leading order, a tendency for ǫ 3 > 0 is observed. With regards to the exact numerical integration, large field models, V (φ) ∝ φ p , with p > 3.1 are now excluded at 95% CL. Small field models, V (φ) ∝ 1 − (φ/µ) p , are still compatible with the data for all values of p. However, if µ/m Pl < 10 is assumed, then the case p = 2 is slightly disfavoured. In addition, mild constraints on the reheating temperature for an extreme equation of state w reh −1/3 are found, namely T reh > 2 TeV at 95% CL. Hybrid models are disfavoured by the data, the best fit model having ∆χ 2 ≃ +5 with two extra parameters in comparison with large field models. Running mass models remain compatible, but no prior independent constraints can be obtained. Finally, superimposed oscillations of trans-Planckian origin are studied. The vanilla slow-roll model is still the most probable one. However, the overall statistical weight in favour of superimposed oscillations has increased in comparison with the WMAP first year data, the amplitude of the oscillations satisfying 2|x|σ 0 < 0.76 at 95% CL. The best fit model leads to an improvement of ∆χ 2 ≃ −12 for 3 extra parameters. Moreover, compared to other oscillatory patterns, the logarithmic shape is favoured.

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Section: Basic Equationsmentioning

confidence: 99%

Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data

Martin

Ringeval

2006

J. Cosmol. Astropart. Phys.

242

374

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“…Should r ≃ 0.01 be observed and ascribed to this scenario, the close proximity of horizon exit to the beginning of inflation would likely imply other observable implications for the CMB, along the lines of those discussed in [216].…”

Section: Model-independent Predictionsmentioning

confidence: 87%

“…This implies thatφ at most rolls through a few Planck scales, which can allow 50 − 60 e -foldings, or even a bit more. This makes the models potentially sensitive to details of the modulus dynamics at horizon exit, along the lines of [216], since this need not be deep in an inflationary regime.…”

Section: Discussionmentioning

confidence: 99%

“…Given the potential sensitivity of inflation to higher-dimension operators, this objection asks why the inflaton potential is not destabilised by integrating out the many heavy particles that are likely to live above the inflationary scale, M I ≃ V 1/4 0 and below the Planck scale? (See, for instance, [216] for more specific variants of this question. )…”

Section: Integrating Out Sub-planckian Modesmentioning

confidence: 99%

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String loop moduli stabilisation and cosmology in IIB flux compactifications

Cicoli¹

2010

Fortschritte der Physik

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We present a detailed review of the moduli stabilisation mechanism and possible cosmological implications of the LARGE Volume Scenario (LVS) that emerges naturally in the context of type IIB Calabi‐Yau flux compactifications. After a quick overview of physics beyond the Standard Model, we present string theory as the most promising candidate for a consistent theory of quantum gravity. We then give a pedagogical introduction to type IIB compactifications on Calabi‐Yau orientifolds where most of the moduli are stabilised by turning on background fluxes. However in order to fix the Kähler moduli one needs to consider several corrections beyond the leading order approximations. After presenting a survey of all the existing solutions to this problem, we derive the topological conditions on an arbitrary Calabi‐Yau to obtain the LVS since it requires no fine‐tuning of the fluxes and provides a natural solution of the hierarchy problem. After performing a systematic study of the behaviour of string loop corrections for general type IIB compactifications, we show how they play a crucial rôle to achieve full Kähler moduli stabilisation in the LVS. Before examining the possible cosmological implication of these scenarios, we present a broad overview of string cosmology. We then notice how, in the case of K3‐fibrations, string loop corrections give rise naturally to an inflationary model which yields observable gravity waves. We finally study the finite‐temperature behaviour of the LVS and discuss prospects for future work.

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“…However, when we say that the stabilized moduli are at the potential minimum, we mean that the zero mode is frozen. The fluctuations around this zero mode could be oscillating about the minimum and this may give rise to interesting effects [9]. In particular, these oscillations could imprint themselves on the CMB power spectrum; it should be noted that the exact nature of the effect depends on the model.…”

Section: Oscillation Effects On the Spectrummentioning

confidence: 99%

Systematics of moduli stabilization, inflationary dynamics and power spectrum

Holman

Hutasoit

2006

J. High Energy Phys.

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Abstract:We study the scalar sector of type IIB superstring theory compactified on Calabi-Yau orientifolds as a place to find a mechanism of inflation in the early universe. In the large volume limit, one can stabilize the moduli in stages using perturbative method. We relate the systematics of moduli stabilization with methods to reduce the number of possible inflatons, which in turn lead to a simpler inflation analysis. Calculating the order-of-magnitude of terms in the equation of motion, we show that the methods are in fact valid. We then give the examples where these methods are used in the literature. We also show that there are effects of noninflaton scalar fields on the scalar power spectrum. For one of the two methods, these effects can be observed with the current precision in experiments, while for the other method, the effects might never be observable.

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Are inflationary predictions sensitive to very high energy physics?

Cited by 161 publications

References 32 publications

Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data

Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data

String loop moduli stabilisation and cosmology in IIB flux compactifications

Systematics of moduli stabilization, inflationary dynamics and power spectrum

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